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2 edition of A Search for 183-GHz emission from water in late-type stars found in the catalog.

A Search for 183-GHz emission from water in late-type stars

A Search for 183-GHz emission from water in late-type stars

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Published by National Aeronautics and Space Administration, Ames Research Center in Moffett Field, Calif .
Written in English

    Subjects:
  • Cool stars,
  • Aerofoils

  • Edition Notes

    Other titlesA search for one hundred eighty three-GHz emission from water in late-type stars
    StatementT.B.H. Kuiper ... [et al.]
    SeriesNASA technical memorandum -- 85987
    ContributionsKuiper, T. B. H, Ames Research Center
    The Physical Object
    FormatMicroform
    Pagination1 v.
    ID Numbers
    Open LibraryOL14926522M

    The physics of water masers observable with ALMA and SOFIA: model predictions for evolved stars. Monthly Notices of the Royal Astronomical Society, Vol. , Issue. 1, p. Monthly Notices of the Royal Astronomical Society, Vol. , Issue. 1, p. Cited by: The Atmosphere: An Introduction to Meteorology (Twelfth Edition) by Frederick K. Lutgens,Edward J. Tarbuck,Dennis Tasa. Pearson Education. 5th or later edition. Softcover. New. Table of Content 1 Introduction to the Atmosphere 2 Heating Earth`s Surface and Atmosphere 3 Temperature 4 Moisture and Atmospheric Stability 5 Forms of Condensation and Precipitation 6 Air Pressure and Winds 7.

    @article{osti_, title = {A STUDY OF RO-VIBRATIONAL OH EMISSION FROM HERBIG Ae/Be STARS}, author = {Brittain, Sean D. and Reynolds, Nickalas and Najita, Joan R. and Carr, John S. and Ádámkovics, Máté}, abstractNote = {We present a study of ro-vibrational OH and CO emission from 21 disks around Herbig Ae/Be stars. We find that the OH and CO luminosities are proportional over a . @article{osti_, title = {Emission from water vapor and absorption from other gases at μm in Spitzer-IRS Spectra Of Protoplanetary Disks}, author = {Sargent, B. A. and Forrest, W. and Watson, Dan M. and Kim, K. H. and Richter, I. and Tayrien, C. and D'Alessio, P. and Calvet, N. and Furlan, E. and Green, J. and Pontoppidan, K., E-mail: [email protected]}, abstractNote = {We present.

    Selective Water Excitation (WE) is different than Fat-Sat, although they are both based around the use of chemically selective RF-pulses. In Fat-Sat, fat protons are selectively excited and then dephased with a spoiler gradient. In WE, fat protons are left alone and water protons are selectively stimulated for . The habitability of red dwarf systems is presumed to be determined by a large number of factors from a variety of sources. Although the low stellar flux, high probability of tidal locking, small circumstellar habitable zones, and high stellar variation experienced by planets of red dwarf stars are impediments to their planetary habitability, the ubiquity and longevity of red dwarfs are factors.


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A Search for 183-GHz emission from water in late-type stars Download PDF EPUB FB2

ABSTRACT A search was made for GHz line emiss~on from water vapour ~n the d~rection of twelve Mira and two semiregular limits to the em~ss~on are in the range of to is estimated that thermal em~ssion from the inner reg~ons of late-type stellar envelopes w~ll be on the order of ten Jy.

A search was made for GHz line emission from water vapor in the direction of twelve Mira and two semiregular variables. Upper limits to the emission are in the range of to Jy. A search was made for GHz line emission from water vapor in the direction of twelve Mira and two semiregular variables.

Upper limits to the emission are in the range of to Jy. It is estimated that thermal emission from the inner regions of late type stellar envelopes will be on the order of ten Jy.

Maser emission, according to one model, would be an order of magnitude by: 2. Get this from a library. A Search for GHz emission from water in late-type stars. [T B H Kuiper; Ames Research Center.;]. A search was made for GHz line emission from water vapor in the direction of twelve Mira and two semiregular variables.

Upper limits to the emission are in the range of to Jy. It is estimated that thermal emission from the inner regions of late type stellar envelopes will be on the order of ten Jy. We have searched for water vapor emission at GHz, redshifted at GHz and GHz, in the two ultraluminous starburst galaxies Mrk and VIIZw SAO/NASA Astrophysics Data System (ADS) Title: A search for GHz emission from water in late-type stars Authors: Kuiper, T.

H., Swanson, P. N., Dickinson, D. The Astrophysics of Emission Line Stars offers general information on emission line stars, starting from a brief introduction to stellar astrophysics, and then moving toward a broad overview of emission line stars including early and late type stars as well as pre-main sequence stars.

Detailed references have been prepared along with an index. Cool Stars, Stellar Systems, and the Sun Broadband linear polarization and chromospheric CA II H and K emission in late-type main sequence stars.

Pages Cool Stars, Stellar Systems, and the Sun Book Subtitle Proceedings of the Fifth Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun Held in Boulder, Colorado, July 7.

Water molecules are also present in interstellar space where they can be formed e.g. in the protection of dust particles (protection against short wavelength radiation).

Even in sunspots water molecules have been detected. Water Masers which are extremely strong sources of water line emission Author: Arnold Hanslmeier.

A search for X-Ray luminous late type stars in NIPSS data.- The Wilson-Bappu relationship - a barometric effect.- Sensitivity of the H.

line to expansion, geometrical extent and temperature gradient in the G and K supergiant chromospheres.- Radio continuum emission from the ionized stellar winds of the cool supergiants in zeta aurigae-like.

The contributions in this volume discuss the magnetic structures in the outer atmospheres of active late-type stars, and in particular the various methods available for imaging surface features on these objects.

Emphasis has been laid upon multiwavelength studies of the phenomena and the application of solar astrophysics to stellar objects. The book is recommended to research workers or. In February, brief observations at GHz were made of Ori MCI as an instrumental check while conducting a se,arch for Gllz emission from late type stars (Kuiper ~ al.

Relative to the previous observations of andthe peak antenna temperature was nearly twice as strong. Emission line stars are attractive to many people because of their spectacular phenomena and their amazing varieties and variability. This book offers general information on emission line stars, starting from a brief introduction to stellar astrophysics and then moving to a broad overview of emission line stars including early and late type stars as well as pre-main sequence Edition: Ed.

Cool Stars, Stellar Systems, and the Sun: Seventh Cambridge Workshop Volume: 26 Year: View this Volume on ADS: Editors: Giampapa, Mark S.; Bookbinder, Jay A. ISBN: eISBN: Electronic access to books and articles. Nucleosynthesis and mixing in low- and intermediate-mass AGB stars.- Abundances in J-type carbon stars.- The abundance of oxygen in M92 giants.- A search for galactic carbon stars.- Surface distribution of M stars with different IRAS colour.- SiO isotope emissions from late-type stars.- Detection of water maser emission from a carbon star V The advent of infrared astronomy has led to the discovery of many luminous.

late-type stars obscured by their circumstellar dust envelope. Sources discovered in the IRC and AFGL infrared sky surveys were followed up by radio observa­ tions, leading to the widespread use of the OH and CO molecules as probes of the circumstellar envelopes.

M-type stars are cool at their surface (~3, K or so) and display strong calcium absorption features since calcium is not ionized at this temperature. - measured by color- stars come in different colors because they emit thermal radiation (go back to light/ energy/ thermal radiation section for more) - i.e.

red stars are cooler than blue stars. Tau Ceti, Latinized from τ Ceti, is a single star in the constellation Cetus that is spectrally similar to the Sun, although it has only about 78% of the Sun's a distance of just under 12 light-years ( parsecs) from the Solar System, it is a relatively nearby star and the closest solitary G-class star.

The star appears stable, with little stellar variation, and is llation: Cetus. Purchase Atmospheric Water Vapor - 1st Edition.

Print Book & E-Book. ISBNBook Edition: 1. Cool Stars, Stellar Systems, and the Sun: Ninth Cambridge Workshop Volume: Year: View this Volume on ADS: Editors: Pallavicini, Roberto; Dupree, Andrea K.

ISBN: eISBN: Electronic access to books and articles is now .The Yerkes spectral classification, also called the MKK system from the authors' initials, is a system of stellar spectral classification introduced in by William Wilson Morgan, Philip C.

Keenan, and Edith Kellman from Yerkes Observatory. This two-dimensional (temperature and luminosity) classification scheme is based on spectral lines sensitive to stellar temperature and surface gravity.A star is an astronomical object consisting of a luminous spheroid of plasma held together by its own nearest star to Earth is the other stars are visible to the naked eye from Earth during the night, appearing as a multitude of fixed luminous points in the sky due to their immense distance from Earth.

Historically, the most prominent stars were grouped into constellations.